GtoChimit:a" Cosmochinrir:a Ar:ta Vol . 56. pp. 3571-3582 OOI6-7037!92!S5.00 + .00 Copyright t. 1992 Perpmon Press Ltd. Printed in U.s.A. Zagami: Product of a two-stage magmatic history TIMOTHY J. Mc CoY, G . JEFFREY TAYLOR, and KLAus KEll Planetary Geosciences, Department of Geology and Geophysics, School of Ocean and Earth Science and Technology, University of Hawaii at Manoa, Honolulu, HI 96822, USA (Received November 14, 1991 ; accepted in revised form June 3,1992) Abstract-Large specimens of the Zagami shergottite show highly varied grain sizes and mineral abun­ dances on a em scale and preferred alignment of pyroxene laths. We document the presence ofwhitlockite and of melt veins and pockets of shock origin. Pyroxene crystals have homogeneous Mg-rich pigeonite and augite cores, overgrown by Fe-rich. zoned pyroxene (mostly pigeonite) rims. Amphibole-bearing magmatic (melt) inclusions occur exclusively in the cores. We conclude that Zagami experienced a two­ stage crystallization history. The first stage occurred in a deep-seated, slowly cooling magma chamber. There, the homogeneous Mg-rich cores of the pyroxenes crystallized during relatively slow cooling. The deep-seated origin of the cores is also indicated by the presence of amphibole within them, which requires pressures of formation equivalent to crystallization at depths> 7.5 km on Mars. Modest abundance of homogeneous Mg-rieh cores ( 15-20%) indicates that crystal settling did not playa significant role in this part of the magma chamber. During the second stage, the Mg-rich pyroxenes were entrained into a magma that either intruded to the near-surface and cooled in a relatively thin dike or sill, or extruded to the surface and crystallized in a lava flow> 10m thick, again without indications for crystal settling. This scenario is suggested by estimates of cooling rates ofO.l-0.5°C/h, based on sizes of the plagioclase (maskelynite) crystals, and of ,....,0.02°C/ h. based on the width of pyroxene exsolution lamellae (BREARLEY, 1991). Irregular shapes of the Mg-rich cores result from resorption and possible solid-state diffusion, and the shapes and sizes of the pyroxenes after crystallization of Fe-rich pigeonite rims onto the cores were strongly controlled by the shapes and sizes of the cores. The finer-grained areas of the rock inherited smaller and more numerous Mg-rich pyroxene cores from the first stage than did the coarser-grained areas. Crystallization of both augite and pigeonite cores at depth, but mostly pigeonite rims in the near­ surface environment, may be the result ofa phase-boundary shift and expansion of the pigeonitc stability field at lower pressures. The estimated depth of the magma chamber for Zagami of> 7.5 km and thickness of the putative lava flow of> 10 m are consistent with calculations and observations of volcanic constructs and flows in the Tharsis region of Mars. INTRODUcrlON shock event that converted the constituent plagioclase into maskelynite, alternative interpretations exist (e.g., JONES, STUDIES OF THE SNC (Shergottites, Nakhlites, Chassignitc) 1986). Petrologic studies of the shergottites have documented meteorites, which are thought to be impact ejecta from the extensive evidence for a major shock event in the history of planet Mars, have contributed significantly to understanding these rocks (e.g., STOFFlER et aI. , 1986). of the igneous history of the planet. The nine SNCs are pet­ Numerous petrologic studies of the shergottites have been rologically diverse. ranging from basalts (shergottites) to py­ camed out to unravel the crystallization histories of these roxenites (nakhlites) to a nearly monomineralic dunite enigmatic rocks, and different investigators have reached (Chassigny). The five shergottites include the remarkably rather different conclusions, Most researchers conclude that similar meteorites Shergotty and Zagami, the layered mete­ crystal settling has played an important role in the igneous orite Elephant Moraine A79001, and the related harzburgites history ortbe shergottites (DUKE, 1968; SM ITH and HERVIG, Allan Hills A77005 and Lewis Cliff 885 16 (ANTARCTIC ME­ 1979; STOLPER and MCSWEE N, 1979; GRIMM and TEORITE NEWSLETTER, 1991). A sixth meteorite originally MCSWEEN, 1982; MCSWEEN, 1985; JAGOUTZ and WANKE, classified as a shergottite (Allan Hills A81313; 0.5 g) has 1986). A number of authors suggested that the shergottites been reclassified as a eucrite (DELANEY and PRINZ, 1989; experienced a one-stage crystallization history (TREIMAN and H. Y. McSween Jr., pers. comm., 1991). SUTTON, 1991) and formed either as shallow intrusives Among the SNCs, the shergottites have probably received (DUKE, 1968; TREIMAN, 1985) or al depth in a magma the most attention,largely because of their drastically different chamber (STOLPER and MCSWEEN, 1979; JAGOUTZ and ages obtained by different isotopic dating techniques and the WANKE, 1986); BREARLEY (1991) comments that Zagami effects that shock may have played in resetting these clocks. formed in a shallow intrusive or, possibly. in a lava flow Isotopic age dating of mineral separates of shergottites by aU significantly thicker than 10 m. Other investigators propose techniques yields internal isochrons near 180 Ma, whereas a a two-stage igneous history for the shergottites inVOlving whole-rock isochron of four shergoUites yields an age of 1.3 crystallization of the homogeneous, Mg-rich pyroxene cores Ga. While the latter age is generally interpreted as the crys­ in a magma chamber and of the Fe-rich, zo ned overgrowths tallization age of these rocks and the former as the age of the on these cores, as well as of the remainder of the rocks in )571 3572 T. J. McCoy, G. J. Taylor, and K. Keil shallow intrusives (SM ITH and HERVIG, 1979; MCSWEEN, their findings here but concentrate on our new observations 1985), perhaps up to 1 km in thickness (GRIM M and and measurements. These new results were made possible by MCSWEEN, 1982). the extraordinarily large samples available to us for study, in We report the results of detailed studies oflarge specimens contrast to the limited sample sizes available to previous of the Zagami shergottile which we conducted as part of a workers. consortium effort on new samples of this meteorite. Hand Sample Descriptions ANALYTICAL TECHNIQUES The two pieces of Zag ami that we obtained weighed 19.5 We studied polished thin sections UNM 991 and 992 of the fin e~ and 352 g. Based on macroscopic appearance, we labelled grained pieces and UNM 993 and 994 of the coa r sc ~grai ned pieces. Quantitative analyses of pyroxene, whitlockite, and shock melt were the larger specimen as fine-grained and the smaller piece as performed on a Cameca Camebax electron microprobe at an accel­ coarse-grained (Fig. 1) although the coarse~grain ed specimen erating potential of 15 keY and an absorbed beam current of20 nA has highly varied grain size, in places identical to the fine~ on Rockport fayalite. Counting times of20 sec were used. Differential grai ned specimen. The larger piece is roughly cubic, 5 cm on matrix effects were corrected using ZAF procedures. A 20 pm broad beam was used to analyze shock melts in order to minimize volatil­ a side, and is covered on one side by black shiny fusion cru st ization. and on fi ve sides by saw cuts. Dark brown, glassy shock vei ns Backscattered electron (BSE) images were taken using an lSI SS~ cut across this specimen. The smaller piece is a sawn slab, 5 40 scanning electron microscope. Photomosaics of portions of thin X 3 X 0.4 cm, and contains glassy pockets. sections UNM 99 1 (fine-grained) and UNM 994 (coarse~grained) were obtained, using many individual BSE images at 30X magnifi~ cation. The finish ed ph otomosaic of a portion of thin section UNM Texture, Grain Size, and Mode 99 1 measures approximately 43 by 30 cm, and that of a portion of thin section UNM 994 measures 54 by 30 em. Mapping of cores was In order to determine the absolute grain sizes and the conducted by hand on the photomosaics. Quantitative analyses of alignment of the constituent minerals more quantitatively, pyroxenes determined the existence of cores in numerous grains we measured four thin sections using the method of DAROT throughout the photomosaic area. Most cores (both their presence (1973), as employed by STOLPER and McSWEEN (1 979) in and extent) were outlined on overlays of the photomosaics by com~ parison with the contrast level of these measured cores. While this their study of Shergotty and Zagami. As di scussed by these subjective assessment introduces some errors, we estimate that our authors, quantitative petrofabric data on shergottites are dif­ volume determinations (both for the bulk rock and individual cores) ficult to obtain because of the existence of two c1inopyroxenes are accurate to within ±5 vol C'"o . The actual volero of cores and their with different optical orientations and the conversion of pla­ areas were measured from our core outlines using digital image pro~ gioclase to isotropic maskelynite. However, the technique of ccssing. The identificat ion of the corcs as either Mg~rich augite or Mg-rich pigeonite was accomplished by semiquantitative electron DAROT (1973) allows an estimate of the degrce of alignment microprobe analysis, using [ sec counts on scalers calibrated on grains of these minerals by counting the number of grain contacts whose precise quantitative compositions were previously dctermined encountered during traverses at various angles to the apparent by conventional electron microprobe techniques. plane of foliation. Minima and maxima in the number of grain contacts correspond to the apparent plane of foliation RESULTS and to the plane perpendicular to it, respectively. The mineralogy and texture of Zag ami has been described Both thin sections of the fine-grained sample have a pro­ previously by a number of authors (c.g., SMITH and HER VIG, nounced alignment of pyroxenes and maskelynite (Fig.